1. The Structure Formation Cookbook 1. Initial Conditions: A Theory for the Origin of Density Perturbations in the Early Universe Primordial Inflation: initial spectrum of density perturbations 2. Cooking with Gravity: Growing Perturbations to Form Structure Set the Oven to Cold (or Hot or Warm) Dark Matter Season with a few Baryons and add Dark Energy 3. Let Cool for 13 Billion years Turn Gas into Stars 4. Tweak (1) and (2) until it tastes like the observed Universe. P m (k)~k n, n~1 P m (k)~T(k)k n P g (k)~b 2 (k)T(k)k n

2. 2 Growth of Large- scale Structure Robustness of the paradigm recommends its use as a Dark Energy probe Price: additional cosmological and structure formation parameters Bonus: additional structure formation parameters

3. 3 Growth of Density PerturbationsVolume Element Flat, matter-dominated w = -0.7 w = –1 Raising w at fixed  DE : decreases growth rate of density perturbations and decreases volume surveyed

4. Sensitivity to Dark Energy equation of state peaks at modest redshift Volume element Comoving distance Huterer & Turner

5. Clusters of Galaxies MS1054, z =0.83 optical image with X-ray overlaid in blue (credit: Donahue) Clusters of galaxies are the largest gravitationally virialized objects in the Universe: M~10 13 -10 15 M sun ~50-90% of their baryonic mass is in the form of intracluster gas The gas is heated as it collapses into the cluster’s gravitational potential well to temperatures of T gas ~ 10 7 -10 8 K The hot intracluster gas emits X-rays and causes the Sunyaev-Zel’dovich (SZ) effect SZ Effect (contours) (OVRO/BIMA) X-ray (color)

6. 6 Clusters form hierarchically z = 7z = 5z = 3 z = 1 z = 0.5z = 0 5 Mpc dark matter time Kravtsov

7. 7 Clusters and Dark Energy MohrVolume Growth (geometry) Number of clusters above observable mass threshold Dark Energy equation of state Requirements 1.Understand formation of dark matter halos 2.Cleanly select massive dark matter halos (galaxy clusters) over a range of redshifts 3.Redshift estimates for each cluster 4.Observable proxy that can be used as cluster mass estimate: p(O|M,z) Primary systematic: Uncertainty in bias & scatter of mass-observable relation

8. 8 Theoretical Abundance of Dark Matter Halos Warren et al ‘05 Warren etal

9. Cluster Mass Function Tinker, Kravtsov et al. 2008, ApJ 688, 709

10. 10 Clusters and Dark Energy MohrVolume Growth (geometry) Number of clusters above observable mass threshold Dark Energy equation of state Requirements 1.Understand formation of dark matter halos 2.Cleanly select massive dark matter halos (galaxy clusters) over a range of redshifts 3.Redshift estimates for each cluster 4.Observable proxy that can be used as cluster mass estimate: p(O|M,z) Primary systematic: Uncertainty in bias & scatter of mass-observable relation

11. 11 Cluster Selection 4 Techniques for Cluster Selection: Optical galaxy concentration Weak Lensing Sunyaev-Zel’dovich effect (SZE) X-ray Cross-compare selection to control systematic errors

12. 12 Holder

13. NSF Site Visit – May 18 - 19, 2009 Relations between observable integrated properties of intracluster gas and cluster mass are expected and observed to be tight, but the amplitude and slope are affected by galaxy formation physics Cluster Scaling Relations “pressure” = Y = gas mass x temperature Nagai 2005; Kravtsov, Vikhlinin, Nagai 2006, ApJ 650, 128 Total cluster mass SZ signal: simulation

14. Cluster SZ Studies Examine clusters at high angular resolution Compare many probes to calibrate SZ signal Simulated Merging Cluster Nagai, Kravtsov, Vikhlinin (2007) SZASZA+CARMA

15. 15 Clusters and Dark Energy MohrVolume Growth (geometry) Number of clusters above observable mass threshold Dark Energy equation of state Requirements 1.Understand formation of dark matter halos 2.Cleanly select massive dark matter halos (galaxy clusters) over a range of redshifts 3.Redshift estimates for each cluster 4.Observable proxy that can be used as cluster mass estimate: p(O|M,z) Primary systematic: Uncertainty in bias & scatter of mass-observable relation

16. 16 Photometric Redshifts Measure relative flux in multiple filters: track the 4000 A break Precision is sufficient for Dark Energy probes, provided error distributions well measured. Redshifted Elliptical galaxy spectrum

17. 17 DES griz DES 10  Limiting Magnitudes g24.6 r24.1 i24.0 z23.9 +2% photometric calibration error added in quadrature Galaxy Photo-z Simulations +VHS* DES griZY +VHS JHKs on ESO VISTA 4-m enhances science reach *Vista Hemisphere Survey Z 23.8 Y 21.6 J 20.3 H 19.4 Ks 18.3

18. 18 Clusters and Dark Energy MohrVolume Growth (geometry) Number of clusters above observable mass threshold Dark Energy equation of state Requirements 1.Understand formation of dark matter halos 2.Cleanly select massive dark matter halos (galaxy clusters) over a range of redshifts 3.Redshift estimates for each cluster 4.Observable proxy that can be used as cluster mass estimate: p(O|M,z) Primary systematic: Uncertainty in bias & scatter of mass-observable relation

19. 19 Precision Cosmology with Clusters? Effect of Uncertainty in mass-observable relation Sensitivity to Mass Threshold Mass threshold

20. 20 Cluster Mass Estimates 4 Techniques for Cluster Mass Estimation: Optical galaxy concentration Weak Lensing Sunyaev-Zel’dovich effect (SZE) X-ray Cross-compare these techniques to reduce systematic errors Additional cross-checks: shape of mass function; cluster correlations (Lima & Hu)

21. Cluster Clustering 21 Clustering amplitude constrains cluster mass